////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7280
SUBJECT: GRB 080210: TAROT La Silla observatory optical detection
DATE: 08/02/10 08:17:14 GMT
FROM: Alain Klotz at CESR-CNRS
Klotz, A. (CESR-OMP), Boer M. (OHP), Atteia J.L. (LATT-OMP) report:
We imaged the field of GRB 080210 detected by SWIFT
(trigger 302888) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.
The observations started 345.9s after the GRB trigger
(11.2s after the notice). The elevation of the field was at
from 15 degrees above horizon and weather conditions
were good.
We detect a new fading source in the error box given by SWIFT
We detected the candidate couterpart not present in the DSS
at the following position (+/- 1 arcsec):
RA(J2000.0) = 16h 45m 03.97s
DEC(J2000.0) +13d 49' 35"
OT was R~16.2 at 345.9s after GRB.
Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.
N.B. Galactic coordinates are lon= 31.6032 lat=+34.1725
and the galactic extinction in R band is 0.2 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.
This message may be cited.
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7281
SUBJECT: GRB 080210: Swift detection of a burst with optical afterglow
DATE: 08/02/10 08:27:08 GMT
FROM: David Palmer at LANL
D. Grupe (PSU), W. H. Baumgartner (GSFC/UMBC), M. M. Chester (PSU),
N. Gehrels (NASA/GSFC), E. A. Hoversten (PSU),
C. B. Markwardt (CRESST/GSFC/UMD), D. M. Palmer (LANL),
A. M. Parsons (GSFC), M. Stamatikos (NASA/ORAU) and M. C. Stroh (PSU)
report on behalf of the Swift Team:
At 07:50:05 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080210 (trigger=302888). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 251.270, +13.830 which is
RA(J2000) = 16h 45m 05s
Dec(J2000) = +13d 49' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a single-peak
with substructure with a duration of about 35 sec. The peak count rate
was ~2000 counts/sec (15-350 keV), at ~10 sec after the trigger. This
was an image trigger, but with a clear light curve.
The XRT began observing the field at 07:54:08 UT, 243 seconds after the
BAT trigger. XRT found a bright, uncatalogued X-ray source
located at RA, Dec 251.2679, +13.8254 which is
RA(J2000) = 16h 45m 04.3s
Dec(J2000) = 13d 49' 31.4"
with an uncertainty of 4.6 arcseconds (radius, 90% containment).
This location is 18.1 arcseconds from the BAT on-board position,
within the BAT error circle.
UVOT took a finding chart exposure of 100 seconds with the White
(160-650 nm) filter starting 160 seconds after the BAT trigger, and
an exposure of 193 seconds with the v filter starting 266 seconds
after the trigger. There is a candidate afterglow in the rapidly
available 2.7'x2.7' sub-image at RA, Dec = 251.2667, +13.8267 (white)
which is
RA(J2000) = 16:45:04.01
DEC(J2000) = +13:49:36.1
with a 1-sigma error radius of about 0.6 arc sec. This position
is 6.3 arcseconds from the center of the XRT error circle. The
estimated magnitude is 18.0 in white and 17.6 in v with
1-sigma errors of about 0.5 mag. The positions agree in both
white and v. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.08.
Burst Advocate for this burst is D. Grupe (grupe AT astro.psu.edu).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7282
SUBJECT: GRB080210 - SDSS Pre-Burst Observations
DATE: 08/02/10 09:00:47 GMT
FROM: Richard J. Cool at U.of AZ/Steward Obs
Richard J. Cool (Arizona), Daniel J. Eisenstein (Arizona), David W. Hogg
(NYU), Michael R. Blanton (NYU), David J. Schlegel (LBNL), J. Brinkmann
(APO),
Donald Q. Lamb (Chicago), Donald P. Schneider (PSU), and Daniel E. Vanden
Berk
(PSU) report:
The Sloan Digital Sky Survey (SDSS) imaged the field of burst GRB080210
prior to the burst. As these data should be useful as a pre-burst comparison
and for calibrating photometry, we are supplying the images and photometry
measurements for this GRB field to the community.
Data from the SDSS, including 5 FITS images, 3 JPGS, and
3 files of photometry and astrometry, are being placed at
http://mizar.as.arizona.edu/~grb/public/GRB080210
We supply FITS images in each of the 5 SDSS bands of a 8'x8' region centered
on the GRB position (ra=251.270 (16:45:04.8), dec=13.8300 (13:49:48.0);
Swift Trigger 302888), as well as 3 gri color-composite JPGs (with different
stretches). The units in the FITS images are nanomaggies per pixel. A pixel
is 0.396 arcsec on a side. A nanomaggie is a flux-density unit equal to
10^-9 of a magnitude 0 source or, to the extent that SDSS is an AB system,
3.631e-6 Jy. The FITS images have WCS astrometric information.
In the file GRB080210_sdss.calstar.dat, we report photometry and astrometry
of 722 bright stars (r<20.5) within 15' of the burst location. The
magnitudes
presented in this file are asinh magnitudes as are standard in the SDSS
(Lupton
1999, AJ, 118, 1406). Beware that some of these stars are not well-detected
in the u-band; use the errors and object flags to monitor data quality.
In the files GRB080210_sdss.objects_flux.dat and
GRB080210_sdss.objects_magnitudes.dat, we report photometry of 1246
objects detected within 6' of the GRB position. We have removed saturated
objects and objects with model magnitudes fainter than 23.0 in the r-band.
The fluxes listed in GRB080210_sdss.objects_flux.dat are in nanomaggies
while the magnitudes listed in GRB080210_sdss.objects_magnitudes.dat are
asinh magnitudes.
**Be aware that at least a portion of the photometry provided in this release
has been flagged as non-photometric. As photometry for objects with this
flag set may have non-optimal calibration, we do not recommend these objects
be used for photometric calibration. Non-photometric imaging may still be
valuable as a pre-burst comparison and for astrometric calibration.
All quantities reported are standard SDSS photometry, meaning that they are
very close to AB zeropoints and magnitudes are quoted in asinh magnitudes.
Photometric zeropoints are known to about 2% rms. None of the photometry
is corrected for dust extinction. The Schlegel, Finkbeiner, and Davis
(1998) predictions for this region are A_U=0.401 mag, A_g=0.295 mag, A_r =
0.214 mag, A_i=0.162 mag, and A_z=0.115 mag.
There are currently no objects within 6 arcminutes of the GRB position in
the SDSS spectroscopic database.
SDSS astrometry is generally better than 0.1 arcsecond per coordinate.
Users requiring high precision astrometry should take note that the SDSS
astrometric system can differ from other systems such as those used in other
notices; we have not checked the offsets in this region.
More detailed information pertaining to our SDSS GRB releases can be found
in our initial data release paper (Cool et al. 2006, PASP 118, 733). See the
SDSS DR4 documentation for more details: http://www.sdss.org/dr5.
These data have been reduced using a slightly different pipeline than that
used for SDSS public data releases. We cannot guarantee that the values here
will exactly match those in the data release in which these data are
included.
In particular, we expect the photometric calibrations to differ by of order
0.01 mag.
This note may be cited, but please also cite the SDSS data release paper,
Adelman-McCarthy et al. (2007, ApJS, 172, 634), when using the data or
referring to the technical documentation.
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7283
SUBJECT: GRB 080210: GOND detection in all bands and redshift upper limit
DATE: 08/02/10 10:06:35 GMT
FROM: Jochen Greiner at MPI
A. Kuepcue Yoldas, A. Yoldas, J. Greiner (all MPE Garching),
S. Klose (Tautenburg Obs), report for the GROND team:
We observed the field of GRB 080210 detected by Swift/BAT (Grupe et al.
2008, GCN 7281) simultaneously in grizJHK with GROND (Greiner et al. 2008,
astro-ph/0801.4801), mounted at the 2.2m MPI/ESO telescope at La Silla (Chile).
Observations started on Feb. 10, at 09:00 UT (1 hr after the GRB),
when the GRB location was becoming visible at 20 degrees above horizon.
We detect the optical afterglow reported by Klotz et al. (2008, GCN 7280)
and Grupe et al. (2008, GCN 7281) in all filters. At 9:02 UT we measure
g'=20.97, r'=19.9, i'=19.61, z'=19.52, J=17.2, H=16.4 and K=15.6, with
errors of +-0.04 in the g'r'i'z' bands, and 0.13 in JHK. The g'-r' color
is consistent with the Ly-break being below the g'-band. Thus, the
redshift is smaller than 3.5, despite the possible expectation from the
long T90 duration of the GRB (and being an image trigger).
The afterglow has clearly faded since the TAROT and UVOT measurements, and
also continues to fade since the start of our observations.
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7284
SUBJECT: GRB 080210: Rapid PROMPT Detections
DATE: 08/02/10 10:21:04 GMT
FROM: Thomas Summers Brennan at UNC/GRB Group
T. Brennan, J. Haislip, D. Reichart, M. Nysewander, A. LaCluyze, K.
Ivarsen, J. A. Crain, A. Foster, M. Schubel, J. Styblova, and A. Trotter
report:
Skynet observed the localization of GRB 080210 (Grupe et al., GCN 7281)
with two of the 16" PROMPT telescopes at CTIO beginning 362 seconds
after the trigger (27 seconds after notification) in VRI.
We detect the afterglow (Klotz et al., GCN 7280) in all filters. At 382
seconds after the burst, we measure V ~ 17.4 mag (calibrated to 2 NOMAD
stars).
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7285
SUBJECT: GRB 080210: Enhanced Swift-XRT position
DATE: 08/02/10 11:56:08 GMT
FROM: Phil Evans at U of Leicester
P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester)
report on behalf of the Swift-XRT team.
Using 193 s of overlapping XRT Photon Counting mode and UVOT
V-band data for GRB 080210, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 251.26693, +13.82656 which is equivalent
to:
RA (J2000): 16h 45m 4.06s
Dec (J2000): +13d 49' 35.6"
with an uncertainty of 2.5 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest position
can be viewed at http://www.swift.ac.uk/xrt_positions. Position enhancement is
described by Goad et al. (2007, astro-ph/0708.0986
http://www.swift.ac.uk/xrt_positions/Goad.pdf).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7286
SUBJECT: GRB 080210: VLT redshift
DATE: 08/02/10 12:22:25 GMT
FROM: Pall Jakobsson at U Hertfordshire
Pall Jakobsson (U. Hertfordshire), Paul M. Vreeswijk, Daniele Malesani
(DARK, NBI), Andreas O. Jaunsen (U. Oslo), Johan P. U. Fynbo, Jens
Hjorth (DARK, NBI) and Nial R. Tanvir (U. Leicester) report on behalf
of a larger collaboration:
Using FORS2 on the Very Large Telescope, we have obtained a 10 min
spectrum (grism 300V) of the optical afterglow of GRB 080210 (Grupe et
al., GCN 7281).
The acquisition image shows the UVOT optical afterglow candidate to
have R = 18.8 on Feb 10.351 UT (0.597 hours after the GRB) using
photometric zeropoints from the ESO webpages. We also obtained an
R-band image at 1.65 hours after the GRB indicating a decay index of
0.76 +/- 0.04.
The spectrum is rich in absorption features, including Ly-alpha, Si II,
C II, Si IV, C IV, Fe II and Al II, corresponding to a redshift of
z = 2.641. This is consistent with the redshift upper limit (z < 3.5)
reported by GROND (Kuepcue Yoldas et al., GCN 7283). There is also a
tentative detection of Ly-alpha in emission superimposed on the DLA
trough.
We thank the Paranal staff for excellent support, especially Paul
Lynam.
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7287
SUBJECT: GRB 080210: Swift-XRT Refined Analysis
DATE: 08/02/10 13:39:47 GMT
FROM: Dirk Grupe at PSU/Swift-XRT
D. Grupe (PSU) reports on behalf of the Swift-XRT Team:
We have analyzed the first 2 orbits of Swift-XRT data obtained for GRB
080210 (Grupe et al. GCN Circ. 7281), totaling 78 s of Windowed Timing
(WT) data and 668 s of Photon Counting (PC) data. The enhanced XRT
position is given in Evans et al. (GCN 7285).
In correction to GCN 7281, XRT started observing the burst 153s after the
trigger.
The X-ray light-curve shows a bright flare at the beginning of the
observations
with an initial decay slope of 7.5+/-0.9 followed by a plateau phase
starting at
290+/-20s after the burst with a decay slope of 0.76+/-0.07.
The WT data (158-232 s after burst) can be modeled as an absorbed
power-law with
photon index of 2.85 ± 0.25 and a free-fit absorbing column of NH =
(21.5 +4.8
-5.4)e20 cm^-2 which is in excess of the Galactic value (5.47e20 cm^-2,
Dickey &
Lockman 1990). The PC mode data are consistent with this result.
Assuming the source continues to decay with the same decay index of 0.76,
we predict an XRT count rate of 0.03 counts/s at T+24 hours, which
corresponds to an 0.3-10.0 keV observed flux of 8.3e-13 ergs cm^-2 s^-1.
This circular is an official product of the Swift-XRT team.
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7288
SUBJECT: GRB 080210: Super-LOTIS observations
DATE: 08/02/10 14:14:49 GMT
FROM: Adria C. Updike at Clemson U
A. C. Updike (Clemson University), G. G. Williams (MMTO), P. A. Milne
(Steward Observatory), and D. H. Hartmann (CU) report on behalf of the
Super-LOTIS Collaboration:
The robotic 0.6-m Super-LOTIS telescope began observing the error box of
GRB 080210 (Swift Trigger 302888, Grupe et al. GCN 7281) at 11:33:46.1 UT,
3 hours and 44 minutes after the trigger. Our observations consist of 57
x 60s exposures in the R-band under good weather conditions.
We detect the afterglow reported by Klotz et al. (GCN 7280) in our stacked
images. Using 5 field stars from the USNO-B1.0 catalogue, we estimate the
following R-band magnitude for the OT:
t_start (UT) exp t (s) t_start-t_0 (s) R Mag
----------------------------------------------------------------
11:33:46.1 3420 11166 R = 21.6 +/- 0.2
Additional observations and analysis are ongoing. This message may be cited.
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7289
SUBJECT: GRB 080210, Swift-BAT refined analysis
DATE: 08/02/10 17:34:35 GMT
FROM: Scott Barthelmy at NASA/GSFC
T. Ukwatta (GWU) S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), D. Grupe (PSU),
H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL),
A. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC)
(i.e. the Swift-BAT team):
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080210 (trigger #302888)
(Grupe, et al., GCN Circ. 7281). The BAT ground-calculated position is
RA, Dec = 251.259, 13.826 deg, which is
RA(J2000) = 16h 45m 02.0s
Dec(J2000) = 13d 49' 35"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 73%.
The mask-weighted light curve shows 3-4 overlapping peaks starting at ~T-16 sec,
peaking at ~T+5 sec, and ending at ~T+33 sec.
T90 (15-350 keV) is 45 +- 11 sec (estimated error including systematics).
The time-averaged spectrum from T-14.6 to T+47.7 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.77 +- 0.12. The fluence in the 15-150 keV band is 1.8 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+4.50 sec in the 15-150 keV band
is 1.6 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence
level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/302888/BA/
[GCN OPS NOTE(10feb08): Per request, AP was added to the author list.]
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7290
SUBJECT: GRB 080210: Hobby-Eberly Telescope Absorption Spectroscopy
DATE: 08/02/10 20:01:00 GMT
FROM: Antonino Cucchiara at PSU
A. Cucchiara and D. B. Fox (PSU) report on behalf of a larger
collaboration:
"Starting on 2008 Feb 10.49 UT we used the Marcario LRS spectrograph
on the Hobby-Eberly Telescope to obtain 2x 1200s spectra of the
optical afterglow (Klotz, Boer & Atteia, GCN 7280) of GRB 080210
(Grupe et al., GCN 7281). The coadded spectrum covers the wavelength
range 4100 to 10,500 Ang. We clearly detect a Ly-alpha absorption
feature as well as several metal features corresponding to FeII, SiII,
CIV, AlII, MnII, the MgII doublet, and MgI at a redshift of z=2.64. No
clear emission lines are evident in our spectrum. Our observations
are consistent with the redshift and features reported by Jakobsson et
al. (GCN 7286). We thank HET Resident Astronomer John Caldwell for
performing this observation."
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7292
SUBJECT: GRB 080210: Swift/UVOT Refined Analysis
DATE: 08/02/11 22:57:46 GMT
FROM: Frank Marshall at GSFC
F.E. Marshall (NASA/GSFC) and D. Grupe (PSU)
report on behalf of the Swift team:
The Swift/UVOT observed the field of GRB 080210 (trigger 302888)
starting 160 seconds after the BAT trigger
(Grupe et al., GCN Circ. 7281), which occurred at 07:50:05 UT.
A bright afterglow was seen in the initial
exposures with the White and V filters
at a position of RA (J2000) of 16h45m04.01s and Dec (J2000) of
+13o49'35.9" (J2000) with an estimated 90% confidence error radius
of 0.6". This position is consistent with the optical
position reported by Klotz et al. (GCN Circ. 7280) and
the enhanced XRT position reported by Evans et al. (GCN Circ. 7285).
There was no 3-sigma detection of the afterglow in
any subsequent exposure in any of the UVOT filters.
The non-detections in the UV filters is consistent with
the redshift of 2.641 reported by Jakobsson et al.
(GCN Circ. 7286). The lack of detection in the second
exposure with the White filter indicates a decay slope
of steeper than -0.7 assuming a power law decay model.
The detections and 3-sigma upper limits in the UVOT photometric
system (Poole et al. MNRAS 383, 627 (2008)) are summarized in
the following table:
Filter T_start(s) T_stop(s) Exposure(s) Mag/3-sigma UL
white 160 260 98 18.2 +/- 0.1
white 6081 6244 161 >20.5
v 267 460 190 17.6 +/- 0.1
b 5877 64094 2625 >21.2
u 5671 69878 4779 >21.3
uvw1 3846 69140 5453 >22.3
uvm2 3639 68241 4447 >21.8
uvw2 9469 74958 4171 >22.3
The values quoted above are not corrected for the expected Galactic
extinction corresponding to a reddening of E(B-V) = 0.08 mag
in the direction of the burst (Schlegel et al. 1998).
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7297
SUBJECT: VLA non-detection of GRB 080210
DATE: 08/02/12 18:15:54 GMT
FROM: Poonam Chandra at U Virginia/NRAO
Poonam Chandra (NRAO/UVA) and Dale A. Frail (NRAO) report on
behalf of the Caltech-NRAO-Carnegie GRB Collaboration:
"We used the Very Large Array to observe the field of view toward
GRB 080210 (GCN 7281) at a frequency of 8.46 GHz on 2008 February
12.53 UT. The radio afterglow of the GRB is undetected at the
Swift-XRT position (GCN 7285). The peak flux at Swift XRT position is
-10+/-43 uJy.
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7298
SUBJECT: GRB 080210: Keck photometry
DATE: 08/02/13 00:12:19 GMT
FROM: Daniel Perley at U.C. Berkeley
D. A. Perley, M. Modjaz, J. S. Bloom, D. Poznanski, A. Miller, and D.
Kocevski (UC Berkeley) report:
On the night of 2008-02-12 (UT), we observed the field of GRB080210
(Grupe et al., GCN 7281) using Keck I (+LRIS) for 600s (R) and 900s (g).
We detect the GRB afterglow at the position noted by Klotz et al. (GCN
7280) and Grupe et al.
Calibrating relative to seven stars from the SDSS calibration table
given in GCN 7282 (Cool et al.), we measure the following magnitudes (at
UT = 15:32, 55.7 hours after the BAT trigger):
R = 24.03 +/- 0.06
g = 25.20 +/- 0.07
The quoted uncertainty is photometric only and does not include scatter
in the field calibration relative to SDSS (which is significant.)
Compared to the photometry given by Updike et al. (GCN 7288) this
suggests an unusually slow decay rate of alpha~0.85. This may suggest
the presence of an underlying host galaxy, but the source appears
pointlike in our images and the redshift of z=2.1 (Jakobbson et al., GCN
7286) would argue against a large host galaxy contribution. The X-ray
afterglow* also appears to be decaying slowly.
---
* http://astro.berkeley.edu/~nat/swift/00302888/bat_xrt.jpg.
////////////////////////////////////////////////////////////////////////
TITLE: GCN CIRCULAR
NUMBER: 7401
SUBJECT: GRB080210: optical observations
DATE: 08/03/10 19:25:26 GMT
FROM: Alexei Pozanenko at IKI, Moscow
E. Klunko (ISTP), A. Pozanenko (IKI) on behalf of larger GRB follow up
collaboration report:
We observed afterglow (Klotz et al. GCN 7280) of GRB080210 (Grupe et al.
GCN 7281) with 1.5m telescope of Sayan observatory (Mondy) on Feb.10
between (UT) 21:36:37 - 22:49:36. The afterglow is marginally detected
(SNR=1.8) in coordinates R.A.(J2000) = 16 45 03.98 Dec.(J2000) = +13 49
35.8. A photometry against USNO-B1.0 is following:
T0+ Exposure R_mag
(mid)
0.594 d 47x60 s 21.8
The afterglow at 0.594d appears ~1 magnitude brighter than expected from a
slow decay rate of alpha ~0.85 (Perley et al. GCN 7298).
The message may be cited.